The Quest for the Missing Dust: New Herschel Maps of Local Group Galaixes (LMC, SMC, M31, M33) that Restore Previously-Missed Extended Emission, Along With SED-Fitting Results, Hydrogen Gas Maps, and Swift Data

Here we provide the data products from publications: Clark, C.J.R., et al., <em>The Quest for the Missing Dust: I – Restoring Large Scale Emission in Herschel Maps of Local Group Galaxies</em>, ApJ 921 35 Clark, C.J.R., et al., <em>The Quest for the Missing Dust: II – Two Orders of Magnitude of Evolution in the Dust-to-Gas Ratio Resolved Within Local Group Galaxies</em>, accepted for publication in ApJ This data concerns four Local Group galaxies: the Large Magellanic Cloud (LMC), the Small Magellanic Cloud (SMC), M31, and M33. For each galaxy, we provide our new Herschel maps, as described in the above publications, which were combined in Fourier space ('feathered') with Planck, IRAS, and COBE data, in order to restore extended emission that was removed from previous Herschel reductions for these galaxies. For each galaxy, we provide this new Herschel data for 5 Hershcel bands: the PACS 100 and 160 \(\mu\)m bands, and the SPIRE 250, 350, and 500 \(\mu\)m bands. This data is provided in FITS format, with one FITS file for each band for each galaxy. Each of these files contains 4 extensions. Extension 1 (IMAGE) provides the standard feathered map. Extension 2 (UNC) provides the uncertainty map. Extension 3 (MASK) provides a binary mask map indicating the portion of the data where reliable, fully-feathered high-resolution coverage is available. Extension 4 provides the foreground-subtracted version of the feathered map (FGND_SUB), the header of which also describes the uncertainty on that subtraction. All maps are in units of MJy/sr (except the MASK extension, which is boolean), We also provide the outputs of our Spectral Energy Distribution (SED) fitting to this data, as described in the publications. For each galaxy, we provide FITS files giving the median value of each parameter in each pixel, and maps of the uncertainties on those medians (being the 68.3% quantile around the median). The parameters are dust mass surface density (Sigma_H.fits), dust temperature (Temp.fits), beta 1 (Beta-1.fits), beta 2 (Beta-2.fits), break wavelength (Break.fits), and 500 \(\mu\)m excess (Excess.fits). Each of these files contain 2 extensions. Extension 1 (median) provides the map of pixel parameter median values. Extension 2 (uncert) provides the map of uncertainties on those medians. Additionally, we provide the full posterior probability distribution for all SED parameters, consisting of 1000 posterior samples, for all pixels, in the form of a FITS file containing a 4-dimensional hypercube, with axes corresponding to right ascension, declination, parameters (in order: dust mass surface density, dust temperature, beta 1, beta 2, break wavelength, and 500 \(\mu\)m excess), and samples. This is provided as a gzip compressed FITS file for each galaxy. For each galaxy, we also provide our maps of the hydrogen surface density (Sigma_H.fits), and dust-to-gas ratio (DtG.fits). Lastly, we provide Swift-UVOT data also used in our analysis. For the LMC and SMC, this is the data presented in Hagen et al. (2017). For M31 and M33, this data was processed in the same manner as the data in Hagen et al. (2017), and will be presented fully in Decleir (in prep.). We provide maps from Swift-UVOT bands W1, W2, and M2. For each band, we provide maps recording the count rate (in photons sec⁻¹), and maps giving the exposure time (in sec), and maps of the surface brightness in MJy sr⁻1 (converted using the Swift-UVOT zero points given in Breeveld et al., 2011).